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Photometric Scaling Relations of Lenticular and Spiral Galaxies

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Photometric Scaling Relations of Lenticular and Spiral Galaxies Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 30 October 2018 (MN LATEX style file v2.2) Photometric scaling relations of lenticular and spiral galaxies E. Laurikainen1⋆, H. Salo1, R. Buta2, J. H. Knapen3,4 and S. Comer´on3,4 1Division of Astronomy, Department of Physical Sciences, University of Oulu, FIN-90014, Finland 2Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 3Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain 4Departamento de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, Spain Accepted: Received: ABSTRACT Photometric scaling relations are studied for S0 galaxies and compared with those obtained for spirals. New two-dimensional multi-component decompositions are pre- sented for 122 early-type disk galaxies, using deep Ks-band images. Combining them with our previous decompositions, the final sample consists of 175 galaxies (Near- Infrared Survey of S0s, NIRS0S: 117 S0s + 22 S0/a and 36 Sa galaxies). As a compar- ison sample we use the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS) of nearly 200 spirals, for which similar multi-component decompositions have previ- ously been made by us. The improved statistics, deep images, and the homogeneous decomposition method used, allows us to re-evaluate the parameters of the bulges and disks. For spirals we largely confirm previous results, which are compared with those obtained for S0s. Our main results are as follows. (1) Important scaling relations are present, indicating that the formative processes of bulges and disks in S0s are coupled o o − (e.g. MK(disk)= 0.63 MK(bulge) 9.3), like has been found previously for spirals (for o o − OSUBSGS spirals MK(disk)= 0.38 MK (bulge) 15.5; the rms deviation from these relations is 0.5 mag, for S0s and spirals). (2) We obtain median reff /hr ∼ 0.20, 0.15 and 0.10 for S0, S0/a-Sa and Sab-Sc galaxies, respectively: these values are smaller than predicted by simulation models in which bulges are formed by galaxy mergers. (3) The properties of bulges of S0s are different from the elliptical galaxies, which is o 0 arXiv:1002.4370v1 [astro-ph.CO] 23 Feb 2010 manifested in the MK(bulge) vs reff relation, in the photometric plane (µ , n, reff ), and to some extent also in the Kormendy relation (<µ>eff vs reff ). The bulges of o − S0s are similar to bulges of spirals with MK(bulge) < 20 mag. Some S0s have small bulges, but their properties are not compatible with the idea that they could evolve to dwarfs by galaxy harassment. (4) The relative bulge flux (B/T ) for S0s covers the full range found in the Hubble sequence, even with 13% having B/T < 0.15, typi- cal for late-type spirals. (5) The values and relations of the parameters of the disks o o (hr, MK(disk), µo(0)) of the S0 galaxies in NIRS0S are similar to those obtained for spirals in the OSUBSGS. Overall, our results support the view that spiral galaxies with bulges brighter than −20 mag in the K-band can evolve directly into S0s, due to stripping of gas followed by truncated star formation. Key words: galaxies: elliptical and lenticular - galaxies: evolution - galaxies: structure ⋆ E-mail: eija.laurikainen@oulu.fi c 0000 RAS 2 E. Laurikainen, H. Salo, R. Buta, J.H. Knapen and S. Comer´on 1 INTRODUCTION The position of S0 galaxies between ellipticals and spirals in galaxy classification schemes (Hubble 1926; de Vaucouleurs 1959; Sandage 1961) has made them of particular interest in any scenario of galaxy formation and evolution. Yet the debate on their origin is open. In the current paradigm, the hierarchical Lambda Cold Dark Matter (ΛCDM) cosmology (Somerville & Primack 1999; Steinmetz & Navarro 2002), the disks are formed first by cooling of gas inside rotating dark matter halos, whereas both the elliptical galaxies and the bulges of disk galaxies are suggested to have formed in major or minor mergers, respectively (Khochfar & Silk 2006). The bulges formed in this manner are dynamically hot and their basic properties were established already in the merger process (Khochfar & Burkert 2005), not affected by the subsequently growing disks. Within ΛCDM, S0s are formed in galaxy mergers in a similar manner as the elliptical galaxies, or they are transformed from spirals which have lost their disk gas by some stripping mechanism (Gunn & Gott 1972; Moore et al. 1996; Bekki, Couch & Shioya 2002). Therefore, it is important to study whether the S0 galaxies are more tightly related to ellipticals or to spirals. However, even if the bulges in S0s were found to be similar to those in spirals, this does not yet answer the question of what the formative processes of bulges in S0s are. It has been suggested that two types of bulges appear: 1) classical merger-built bulges, and 2) disk-like bulges formed by star formation in the disk (Kormendy 1982; see also review by Kormendy & Kennicutt 2004). Boxy/peanut bulges are often listed as a separate class, but as they are assumed to be part of a bar (Athanassoula, Lambert & Dehnen 2005), they are basically disk-related structures. Bulges in late-type spirals are typically photometrically disk-like (Andredakis & Sanders 1994; Carollo et al., 1997, 1998) rotationally supported structures (Cappellari et al. 2007), whereas for the bulges of early-type spirals contradictory results have been obtained. In particular, the fairly large masses of the bulges in the early-type galaxies are difficult to explain by secular evolution alone, related to bar-induced gas infall and subsequent star formation in the central regions of the galaxies (see Kormendy & Kennicutt 2004), at least if no external intergalactic material is added to the bulge. It needs to be re-investigated what is the nature of bulges of S0s in the nearby Universe, e.g. are they disk-like or more likely have properties of merger built structures. Answering this question would set important constraints on models of galaxy formation and evolution. Scaling relations have been used for theoretical modeling of elliptical galaxies (see de Zeeuw & Franx 1991), and for eval- uating the formation of galactic disks in spiral galaxies (Dalcanton, Spergel & Summers 1997; Firmani & Avila-Rees 2000). Therefore, the scaling relations can be used as a tool to study the origin of S0s, which morphologically appear between the two main types of galaxies. One such scaling relation was introduced by Kormendy (1977), who showed, using R1/4 models, that the effective radius (reff ) is connected to the central surface brightness (µ0), both for elliptical galaxies and for bulges of early- type disk galaxies. The dispersion in this so-called Kormendy relation is reduced by adding a third parameter, a S´ersic index n, leading to the photometric plane (e.g. Khosroshahi, Wadadekar & Kembhavi 2000). Alternatively, if the central velocity dis- persion is used, the fundamental plane is obtained (e.g. Djorgovski & Davis 1987; Dressler et al. 1987). Other important scaling relations appear between the brightnesses and the scale parameters of the bulge and the disk (Courteau, de Jong & Broeils 1996), and between the brightness of the bulge with the total galaxy brightness (Yoshizawa & Wakamatsu 1975; Carollo et al. 2007). The scaling relations studied for the S0 galaxies so far are open to different interpretations: while the fundamental plane and the Kormendy relation have associated their bulges with the elliptical galaxies (Pahre, Djorgovski & Carvalho 1998; Pierini et al. 2002; Aguerri et al. 2005a), the scale parameters of the bulge and the disk hint to a spiral origin (Aguerri et al. 2005a; Laurikainen et al. 2009). In a broader context, scaling relations for spiral galaxy samples have been extensively studied revealing several fundamental relations (see Ravikumar et al. 2006; Graham & Worley 2008 as some of the latest works). However, the spiral samples contain just a small number of S0s, which makes it difficult to draw conclusions about S0 properties. In addition, except for the first attempts by Aguerri et al. (2005a) and Laurikainen et al. (2009), the scaling relations for the disk galaxies have not yet been studied using a 2D multi-component approach, which is important in accounting for structure, particularly in barred disk galaxies (Peng 2002; Laurikainen et al. 2004, 2006; Gadotti 2008). In this study the photometric scaling relations are studied for a sample of 175 early-type disk galaxies, mainly S0s in NIRS0S. This is the largest sample of S0s studied in detail up to now. We use deep Ks-band images for decomposing the two-dimensional surface brightness image to structure components, including bars, ovals and lenses. We present new decompositions for 122 galaxies, and use our previously published decompositions for the rest of the NIRS0S sample. As a comparison sample we use the Ohio State University Bright Spiral Galaxy survey (OSUBSGS; Eskridge et al. 2002) of nearly 200 spirals, for which similar multi-component decompositions have been previously made by us (Laurikainen et al. 2004). Our main emphasis is to compare whether the photometric properties of bulges in S0s are more similar to those of elliptical galaxies or bulges in spirals. Also, implications of these scaling relations for the formative processes of bulges in S0s are discussed. Our uniform decomposition approach, applied for a statistically significant sample of galaxies, using deep Ks-band images, allows us to re-evaluate the properties of bulges and disks in S0s, and to make an unbiased comparison with spirals. c 0000 RAS, MNRAS 000, 000–000 Photometric scaling relations of NIRS0S and OSUBSGS samples 3 2 SAMPLE AND OBSERVATIONS Our primary sample consists of 175 early-type disk galaxies, mainly S0s (117 S0s, 22 S0/a-Sa, 36 Sa galaxies).
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